Computational Astrophysics · Interactive Learning Module
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This module uses the same login, tab, simulation, data, quiz, and reference architecture as the first simulator for course-wide uniformity. The present engine is fully optical-depth specific and models attenuation in dusty interstellar media.
Optical depth quantifies attenuation through absorbing or scattering media.
As optical depth increases, transmitted intensity decreases exponentially.
Dust extinction is wavelength dependent and generally stronger at shorter wavelengths.
Here \(N\) is a dust-column scale factor, \( \kappa_0 \) is the opacity normalization, \( \beta \) controls the slope of the dust law, and \(L\) is a path-length scale.
These limits determine whether radiation escapes almost freely or is strongly suppressed.
Optical depth is central to dust lanes, molecular clouds, circumstellar shells, and embedded star-forming regions.
Because blue light is often attenuated more than red light, dusty objects appear reddened. This connects directly to extinction curves and observed stellar colors.
CSV columns: sapid, student_name, runtime_s, N, k0, beta, L, ref_lambda_nm, tau_ref, trans_ref, mean_tau, mean_transmission.
| Runtime (s) | N | k0 | beta | L | Ref λ (nm) | tau ref | T ref | Mean tau | Mean T |
|---|---|---|---|---|---|---|---|---|---|
| No data yet — run the simulation with log data checked. | |||||||||
| Timestamp (ISO) | Name | SAPID |
|---|---|---|
| No login records yet. | ||
This module targets Unit 4 of PHYS4022P. Students model wavelength-dependent attenuation through interstellar dust and connect simulated outputs to observational interpretation.